A population of faint, old, and massive quiescent galaxies at [Formula: see text] revealed by JWST NIRSpec Spectroscopy.

Autor: Nanayakkara T; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC, 3122, Australia. wnanayakkara@swin.edu.au., Glazebrook K; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC, 3122, Australia., Jacobs C; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC, 3122, Australia., Kawinwanichakij L; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC, 3122, Australia., Schreiber C; IBEX Innovations, Sedgefield, Stockton-on-Tees, TS21 3FF, UK., Brammer G; Cosmic DAWN Center, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200, Copenhagen N, Denmark., Esdaile J; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC, 3122, Australia., Kacprzak GG; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC, 3122, Australia., Labbe I; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218, Hawthorn, VIC, 3122, Australia., Lagos C; Cosmic DAWN Center, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200, Copenhagen N, Denmark.; ARC Centre for Excellence in All-Sky Astrophysics in 3D, Canberra, Australia.; International Centre for Radio Astronomy Research, University of Western Australia, 7 Fairway, Crawley, 6009, WA, Australia., Marchesini D; Physics and Astronomy Department, Tufts University, 574 Boston Avenue, Medford, MA, 02155, USA., Marsan ZC; Department of Physics and Astronomy, York University, 4700 Keele Street, Toronto, ON, M3J 1P3, Canada., Oesch PA; Cosmic DAWN Center, Niels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200, Copenhagen N, Denmark.; Department of Astronomy, University of Geneva, Chemin Pegasi 51, 1290, Versoix, Switzerland., Papovich C; Department of Physics and Astronomy, and George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A &M University, College Station, TX, 77843-4242, USA., Remus RS; University Observatory Munich, Faculty of Physics, Ludwig-Maximilians-University, Scheinerstrasse 1, 81679, Munich, Germany., Tran KH; School of Physics, University of New South Wales, Kensington, Australia.; ARC Centre for Excellence in All-Sky Astrophysics in 3D, Canberra, Australia.; Center for Astrophysics, Harvard & Smithsonian, Cambridge, MA, USA.
Jazyk: angličtina
Zdroj: Scientific reports [Sci Rep] 2024 Feb 14; Vol. 14 (1), pp. 3724. Date of Electronic Publication: 2024 Feb 14.
DOI: 10.1038/s41598-024-52585-4
Abstrakt: Here we present a sample of 12 massive quiescent galaxy candidates at [Formula: see text] observed with the James Webb Space Telescope (JWST) Near Infrared Spectrograph (NIRSpec). These galaxies were pre-selected from the Hubble Space Telescope imaging and 10 of our sources were unable to be spectroscopically confirmed by ground based spectroscopy. By combining spectroscopic data from NIRSpec with multi-wavelength imaging data from the JWST Near Infrared Camera (NIRCam), we analyse their stellar populations and their formation histories. We find that all of our galaxies classify as quiescent based on the reconstruction of their star formation histories but show a variety of quenching timescales and ages. All our galaxies are massive ([Formula: see text] M[Formula: see text]), with masses comparable to massive galaxies in the local Universe. We find that the oldest galaxy in our sample formed [Formula: see text] M[Formula: see text] of mass within the first few hundred million years of the Universe and has been quenched for more than a billion years by the time of observation at [Formula: see text] ([Formula: see text] billion years after the Big Bang). Our results point to very early formation of massive galaxies requiring a high conversion rate of baryons to stars in the early Universe.
(© 2024. Crown.)
Databáze: MEDLINE
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